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There is an emerging consensus that large amounts of gas do not shock heat inthe circumgalactic medium (CGM) of massive galaxies, but instead pierce deepinto haloes from the cosmic web via filaments. To better resolve this processnumerically, we have developed a novel `shock refinement' scheme within themoving mesh code AREPO that adaptively improves resolution around shockson-the-fly in galaxy formation simulations. We apply this to a massive$\sim10^{12}$ M$_\odot$ halo at $z=6$ using the successful FABLE model,increasing the mass resolution by a factor of 512. With better refinement thereare significantly more dense, metal-poor and fast-moving filaments and clumpsflowing into the halo, leading to a more multiphase CGM. We find a $\sim50$ percent boost in cool-dense gas mass and a 25 per cent increase in inflowing massflux. Better resolved accretion shocks cause turbulence to increasedramatically, leading to a doubling in the halo's non-thermal pressure support.Despite much higher thermalisation at shocks with higher resolution, increasedcooling rates suppress the thermal energy of the halo. In contrast, the fasterand denser filaments cause a significant jump in the bulk kinetic energy ofcool-dense gas, while in the hot phase turbulent energy increases by up to$\sim150$ per cent. Moreover, HI covering fractions within the CGM increase byup to 60 per cent. Consequently star formation is spread more widely and wepredict a population of metal-poor stars forming within primordial filamentsthat deep JWST observations may be able to probe.

Resolving shocks and filaments in galaxy formation simulations: effects on gas properties and star formation in the circumgalactic medium